Mass versus size distribution of the ALMA-IMF cores, compared, for reference, to the mass-size relation of critical Bonnor-Ebert spheres for T_dust = 20 K (continuous line) and the location of 90% of the core sample of Könyves et al. (2015) and Sanhueza et al. (2019) (dark and light gray shaded areas at the bottom-right corner). The median (open markers) and 1σ dispersion (error bars) of the core distributions for each group of Young (green), Intermediate (orange), and Evolved (red) protocluster clouds are relatively homogeneous. The core FWHMs are deconvolved from the beams, where the minimum deconvolved size corresponds to a half-beam angular diameter and the largest cores are not necessarily the most massive.