We utilize ALMA archival data to estimate the dust disk size of 152 protoplanetary disks in Lupus (1-3Myr), Chamaeleon I (2-3Myr), and Upper-Sco (5-11Myr). We combine our sample with 47 disks from Tau/Aur and Oph whose dust disk radii were estimated, as here, through fitting radial profile models to visibility data. We use these 199 homogeneously derived disk sizes to identify empirical disk-disk and disk-host property relations as well as to search for evolutionary trends. In agreement with previous studies, we find that dust disk sizes and millimeter luminosities are correlated, but show for the first time that the relationship is not universal between regions. We find that disks in the 2-3Myr old ChaI are not smaller than disks in other regions of similar age, and confirm the Barenfeld et al. finding that the 5-10Myr USco disks are smaller than disks belonging to younger regions. Finally, we find that the outer edge of the solar system, as defined by the Kuiper Belt, is consistent with a population of dust disk sizes which have not experienced significant truncation.