Shocks are a crucial probe to understanding the ongoing chemistry within ices on interstellar dust grains, where many complex organic molecules (COMs) are believed to be formed. However, previous theoretical work has been limited to the initial liberation into the gas-phase through non-thermal desorption processes such as sputtering. Here, we present results from an adaptation of the three-phase gas-grain chemical network code, NAUTILUS, with the inclusion of additional high-temperature reactions, non-thermal desorption, collisional dust heating, and shock-physics parameters. From this, we are able to reproduce many of the conclusions by Burkhardt et al. (2016) through observations of the prototypical shocked-outflow L1157. In particular, we have shown that gas-phase CH$_3$OH is primarily enhanced through solely sputtering and gas-phase HNCO is significantly enhanced by both sputtering and post-shock chemistry. In addition, we find that NH$_2$CHO has a significant post-shock chemistry formation route, differing from many other COMs observed in shocks. We will also discuss the potential dependence of sulfur-chemistry on shocks and its usefulness as a shock tracer in protoplanetary disks. Finally, we will introduce the ongoing efforts to constrain this model through single-dish and interferometric observations of a wide variety of shocked outflows.