We have conducted observations toward the molecular cloud associated with the H II region Sh 156 in 13CO(J = 1-0), C18O(J = 1-0), and CS(J = 2 -1) using the TRAO 14 m telescope. Combining with existing 12CO(J = 1- 0) data of the Outer Galaxy Survey, we delineated the physical properties of the cloud. We found that there is a significant sign of interaction between the H II region and the molecular gas. We estimated the masses of the molecular cloud, using three different techniques; the most plausible mass is estimated to be 1.37 X 105M⊙, using a conversion factor of X = 1.9 X 1020cm-2 (K km s-1)-1, and this is similar to virial mass estimate. This implies that the cloud is gravitationally bound and in virial equilibrium even though it is closely associated with the H II region. In addition to existing outflow, we found several MSX and IRAS point sources associated with dense core regions. Thus, more star forming activities other than the existing H II region are also going on in this region.