as it does not self-shield like the H$_2$ molecule. Therefore, there is less CO compared to the H$_2$ abundance in the Magellanic Clouds than in the Galaxy. This translates into higher values of $X_{\textrm{CO}}$ in the LMC compared to the Galaxy. In general the conversion factor increases with higher radiation fields and decreases with higher metallicities. We adopt the median conversion factor in the LMC compiled from the literature by Bolatto et al. (2013) of $$X_{\textrm{CO}} = 8.8 \pm 0.3 \times 10^{20} \,[\textrm{cm}^{-2} \textrm{(K kms}^{-1})^{-1}].$$ The adopted $X_{\textrm{CO}}$ factor is 3.8 times larger than the canonical Galactic $X_{\textrm{CO}}$ of Bolatto et al. (2013). Our adopted value is similar to that found by Herrera et al. (2013) when comparing molecular and dust mass estimates in the LMC N11 region; but higher than the value of $6 \times 10^{20} \,\textrm{cm}^{-2} \textrm{(K kms}^{-1})^{-1}$ reported by Roman-Duval et al. (2014). The resulting cloud masses if we adopted the Roman-Duval et al. (2014) $X_{\textrm{CO}}$ would be reduced by $\sim20$%.

### Virial mass

The virial mass ($M_{\rm{vir}}$) was computed assuming that each cloud is spherical, is in virial equilibrium and has a density ($\rho$) profile of the form $\rho \propto
r^{-1}$. The virial mass is given 