Relationships between physical properties of our sample, together with results in this same region found in Kalari et al. (2018), in 30 Dor from Wong et al. (2022) with ~ 1″ resolution, in the LMC from Wong et al. (2011 ), in Milky Way clouds from Heyer et al. (2009) and inner Galaxy dense clumps from ATLASGAL (Urquhart et al. 2018). Our CPROPS clumps are shown in red and black in both plots. The filled circles represent completely resolved clumps, whereas the empty diamonds correspond to clumps that have one unresolved axis. Left: R vs σ_v relationship for molecular clouds in the LMC and the Milky Way. The black line represents the canonical relation σ_v = 0.72R^0.5, followed by the Milky Way clouds (Solomon et al. 1987), whereas the dash-dotted line marks the relation found in Wong et al. (2022). Right: ${\sigma }_v^2/R$ vs Σ_H2 relationship for molecular clouds in different galaxies, including our results and other regions in 30 Dor, the LMC, and the Milky Way. The solid black line represents the approximate ${\sigma }_v^2/R$ value for increasing ${\mathrm{\Sigma }}_{H_2}$ of a centrally concentrated, virialized clump confined only by self-gravity. The dashed lines represent the relation between ${\sigma }_v^2/R$ and ${\mathrm{\Sigma }}_{H_2}$ for clumps with σ_v affected by self-gravity and external pressure, covering the range P/k_B = 10³-10⁹ cm^-3 K (Field et al. 2011).