Abstract: We selected 67 relatively isolated massive star-forming clumps and studied their overall chemical properties using four molecular spectral lines (HCN(1-0), HNC(1-0), HCO⁺(1-0), and CN(1-0), where the numbers in parentheses represent the transition from rotational energy level 1 to rotational energy level 0) and infrared band data. Based on the statistics of the source's integral intensity, column density, molecular abundance and abundance ratio at different evolutionary stages, we found that the median values of the integral intensity and column density of the massive star forming clumps CN(1-0), HCO⁺(1-0), HCN(1-0) and HNC(1-0) all showed an increasing trend with the increase of the evolutionary stage, which is consistent with the theoretical expectation. However, the statistical results of column density and abundance based on a single molecule have large errors. The stage of evolution used to trace is very limited. The integral intensity ratio of I(CN)/ I(HNC), I(CN)/ I(HCN) and I(HCN)/ I(HCO⁺) increases with the evolution stage ( I represents the integrated intensity of the molecule), which is a potential probe to trace the evolution of massive star forming clumps. The median values of N(CN)/ N(H₂),N(HNC)/N(H_2) and N(HCN)/N(HCO⁺) increase monotonically with the evolution stage (N represents the column density of the molecule), which is promising as a chemical probe to trace the evolution of massive stars. It should be noted that due to the limitations of the observational data in this study, optical depths of individual molecules cannot be obtained. As a result, reliable column densities and abundances cannot be determined, which ultimately affects the testing of abundance ratio chemical clocks.