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We compare the observational properties between ^12 CO, ^13 CO, and C ^18 O and summarize the observational parameters based on a 7069-cloud sample from the Milky Way Imaging Scroll Painting CO survey in a section of the third Galactic quadrant. We find that the ^13 CO angular area ( ${A}_{{}^{13}\mathrm{CO}}$ ) generally increases with that of ^12 CO ( ${A}_{{}^{12}\mathrm{CO}}$ ), and the ratio of ${A}_{{}^{13}\mathrm{CO}}$ to ${A}_{{}^{12}\mathrm{CO}}$ is 0.38 by linear fitting. We find that the ^12 CO and ^13 CO flux are tightly correlated as ${F}_{{}^{13}\mathrm{CO}}=0.17\,{F}_{{}^{12}\mathrm{CO}}$ with both fluxes calculated within the ^13 CO-bright region. This indicates that the abundance ${X}_{{}^{13}\mathrm{CO}}$ is a constant as ${6.5}_{-0.5}^{+0.1}\times {10}^{-7}$ for all samples under the assumption of local thermodynamic equilibrium (LTE). Additionally, we observed that the X-factor is approximately constant in a large sample of molecular clouds. Similarly, we find ${F}_{{{\rm{C}}}^{18}{\rm{O}}}=0.11\,{F}_{{}^{13}\mathrm{CO}}$ with both fluxes calculated within the C ^18 O-bright region, which indicates that the abundance ratio ${X}_{{}^{13}\mathrm{CO}}/{X}_{{{\rm{C}}}^{18}{\rm{O}}}$ stays at the same value of ${9.7}_{-0.8}^{+0.6}$ across the molecular clouds under the LTE assumption. The linear relationships of ${F}_{{}^{12}\mathrm{CO}}$ versus ${F}_{{}^{13}\mathrm{CO}}$ and ${F}_{{}^{13}\mathrm{CO}}$ versus ${F}_{{{\rm{C}}}^{18}{\rm{O}}}$ hold not only for the ^13 CO-bright region and C ^18 O-bright region, but also for the entire molecular cloud scale with a lower flux ratio. The abundance ratio ${X}_{{}^{13}\mathrm{CO}}/{X}_{{{\rm{C}}}^{18}{\rm{O}}}$ inside the clouds shows a strong correlation with the column density and temperature. This indicates that the ratio ${X}_{{}^{13}\mathrm{CO}}/{X}_{{{\rm{C}}}^{18}{\rm{O}}}$ is dominated by a combination of chemical fractionation, selective dissociation, and the self-shielding effect inside the clouds.