The paper presents a method to assess the quality of dynamical measurements of protoplanetary disk gas masses using resolved (CO) spectral line data. The authors designed controlled injection and recovery experiments to develop an analysis prescription that accounts for observational limitations, measurement biases, and geometric and physical uncertainties. The approach performed well for massive disks ($M_d/M_* = 0.1$), with inferred $M_d$ posteriors recovering true values with little bias ($\lesssim 20\%$) and uncertainties within a factor of two ($2\sigma$). The gas surface density profiles were also recovered with high fidelity. However, the approach becomes insensitive when $M_d/M_* \lesssim 5\%$, due to degeneracies in surface density profile parameters. Including multiple lines and improving associated tools might push this boundary down by another factor of $\sim$two in ideal scenarios. The authors demonstrated the approach using archival ALMA observations of the MWC 480 disk, measuring $M_d = 0.13_{-0.04}^{+0.04} M_{\odot}$ and identifying kinematic substructures consistent with surface density gaps. Overall, the study suggests that these dynamical measurements offer powerful constraints on gas masses and surface densities, serving as key benchmarks for detailed thermo-chemical modeling. The paper also discusses prospects for improvements and various caveats and limitations.The paper presents a method to assess the quality of dynamical measurements of protoplanetary disk gas masses using resolved (CO) spectral line data. The authors designed controlled injection and recovery experiments to develop an analysis prescription that accounts for observational limitations, measurement biases, and geometric and physical uncertainties. The approach performed well for massive disks ($M_d/M_* = 0.1$), with inferred $M_d$ posteriors recovering true values with little bias ($\lesssim 20\%$) and uncertainties within a factor of two ($2\sigma$). The gas surface density profiles were also recovered with high fidelity. However, the approach becomes insensitive when $M_d/M_* \lesssim 5\%$, due to degeneracies in surface density profile parameters. Including multiple lines and improving associated tools might push this boundary down by another factor of $\sim$two in ideal scenarios. The authors demonstrated the approach using archival ALMA observations of the MWC 480 disk, measuring $M_d = 0.13_{-0.04}^{+0.04} M_{\odot}$ and identifying kinematic substructures consistent with surface density gaps. Overall, the study suggests that these dynamical measurements offer powerful constraints on gas masses and surface densities, serving as key benchmarks for detailed thermo-chemical modeling. The paper also discusses prospects for improvements and various caveats and limitations.