Collisions between giant molecular clouds (GMCs) have been proposed as a mechanism to trigger star formation in galaxies. The theory has been considered as a candidate explaining the star formation rate and star formation efficiency. The dense structures formed in the procedure can also be the precursors of mass stars and star clusters. Recently, more and more observations are planned to search the evidences of cloud-cloud collusion from the molecular emission lines, such as SiO. To analyze the signals and interpret the local kinematic/chemical properties, we follow the previous simulation works and set magnetohydrodynamics coupling with astrochemical network to study the chemical evolution during the process. The results can help us estimate the magnetic field, cosmic ray, etc in infrared dark clouds (IRDCs) and thus study the formation of massive stars and star clusters.