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The ability of young stellar clusters to expel or retain the gas left overafter a first episode of star formation is a central issue in all models aimingto explain multiple stellar populations and the peculiar light elementabundance patterns in globular clusters. Recent attempts to detect the gas leftover from star formation in present day clusters with masses similar to thoseof globular clusters did not reveal a significant amount of gas in the majorityof them, which strongly restricts the scenarios of multiple stellar populationformation. Here the conditions required to retain the gas left over from starformation within the natal star forming cloud are revised. It is shown that theusually accepted concept regarding the thermalization of the star clusterkinetic energy due to nearby stellar winds and SNe ejecta collisions must betaken with care in the case of very compact and dense star forming clouds wherethree star formation regimes are possible if one considers different starformation efficiencies and mass concentrations. The three possible regimes arewell separated in the half-mass radius and in the natal gas central density vspre-stellar cloud mass parameter space. The two gas free clusters in theAntennae galaxies and the gas rich cluster with a similar mass and age in thegalaxy NGC 5253 appear in different zones in these diagrams. The critical linesobtained for clusters with a solar and a primordial gas metallicity arecompared.

Gas expulsion vs gas retention: what process dominates in young massive clusters?