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Studies based on Hubble Space Telescope ($HST$) photometry in F275W, F336W,and F438W have shown that the incidence and complexity of multiple populations(MPs) in Globular Clusters (GCs) depend on cluster mass. This result, however,is based on nearby, low-reddening Galactic GCs, for which we can obtainaccurate F275W photometry. In this work we exploit $HST$ photometry in F336W,F438W, and F814W to characterize MPs in 68 Galactic and extragalactic GCs byusing the pseudo-color $C_{F336W,F438W,F814W}$, which is more efficient interms of observation time than the pseudo-color $C_{F275W,F336W,F438W}$ adoptedin previous works. We first analyzed the Galactic GCs alone and find that theRGB color width strongly correlates with [Fe/H]. After removing the dependencefrom metallicity, we obtain a strong correlation with cluster mass, thusconfirming previous findings. We then exploited the RGB width to compare MPs inGalactic and extragalactic GCs. Similarly to Galactic GCs, the RGB width ofMagellanic Cloud GCs correlates with clusters mass, after removing thedependence from metallicity. This fact demonstrates that cluster mass is themain factor affecting the properties of MPs. Magellanic Cloud clusters exhibit,on average, narrower RGBs than Galactic GCs with similar mass and metallicity.We suggest that this difference is a signature of stellar mass loss in GalacticGCs. As an alternative, the mass-RGB-width relation would depend on the hostgalaxy. Finally, we used ground-based photometry to investigate Terzan\,7through the $C_{U,B,I}$ pseudo-color, ground-based analogous of$C_{F336W,F438W,F814W}$, and find that this cluster is consistent with a simplepopulation.

The role of cluster mass in the multiple populations of Galactic and extragalactic globular clusters