We present analyses of 1250 variable sources identied in a 20 square degree eld toward NGC 2784 by the KMTNet Supernova Program. We categorize the variable sources into three groups based on their B-band variability. The rst group consists of 31 high variability sources with their B- band RMS variability greater than 0.3 magnitudes. The second group of medium variability contains 265 sources with RMS variability between 0.05 and 0.3 magnitudes. The remaining 951 sources belong to the third group of low variability with an RMS variability smaller than 0.05 magnitudes. Of the entire 1250 sources, 4 clearly show periods of variability greater than 100 days, while the rest have periods shorter than 51 days or no reliable periods. The majority of the sources show either rather irregular variability or short periods faster than 2 days. Most of the sources with reliable period determination between 2 and 51 days belong to the low-variability group, although a few belong to the medium-variability group. All the variable sources with periods longer than 35 days appear to be very red with B􀀀V > 1.5 and V 􀀀I > 2.1 magnitudes. We classify candidates of 51 Cepheids, 17 semi-regular variables, 3 Mira types, 2 RV(B) Tauri stars, 26 eclipsing binary systems and 1 active galactic nucleus. The majority of long-term variables in our sample belong to either Mira or semi-regular types, indicating that long-term variability may be more prominent in post-main sequence phases of late-type stars. The depth of the eclipsing dips of the 26 candidates for eclipsing binaries is equivalent to 0.61 as the average relative size of the two stars in the binary system. Our results illustrate the power of the KMTNet Supernova Program for future studies of variable objects.

Abstract
1. INTRODUCTION
2. OBSERVATIONS AND DATA
3. VARIABILITY, COLOR AND PERIOD
4. CLASSIFICATIONS AND VARIABLE TYPES
5. SUMMARY AND CONCLUSION
REFERENCES

• Matthias Yang He(Department of Astronomy and Astrophysics, University of Toronto/The Pennsylvania State University) Corresponding author
• Dae-Sik Moon(Department of Astronomy and Astrophysics, University of Toronto)
• Hilding Neilson(Department of Astronomy and Astrophysics, University of Toronto)
• Jae-Joon Lee(Korea Astronomy and Space Science Institute)
• Sang Chul Kim(Korea Astronomy and Space Science Institute/Korea University of Science and Technology)
• Mina Pak(Korea Astronomy and Space Science Institute/Korea University of Science and Technology)
• Hong Soo Park(Korea Astronomy and Space Science Institute/Korea University of Science and Technology)
• Dong-Jin Kim(Korea Astronomy and Space Science Institute)
• Yongseok Lee(Korea Astronomy and Space Science Institute/School of Space Research, Kyung Hee University)
• Seung-Lee Kim(Korea Astronomy and Space Science Institute/Korea University of Science and Technology)
• Chung-Uk Lee(Korea Astronomy and Space Science Institute/Korea University of Science and Technology)