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Intermediate-age star clusters in the Magellanic Clouds harbour signatures ofthe multiple stellar populations long thought to be restricted to old globularclusters. We compare synthetic horizontal branch models with Hubble SpaceTelescope photometry of clusters in the Magellanic Clouds, with age between ~2and ~10 Gyr, namely NGC 121, Lindsay 1, NGC 339, NGC 416, Lindsay 38, Lindsay113, Hodge 6 and NGC 1978. We find a clear signature of initial heliumabundance spreads (delta(Y)) in four out of these eight clusters (NGC 121,Lindsay 1, NGC 339, NGC 416) and we quantify the value of delta(Y). For twoclusters (Lindsay 38, Lindsay 113) we can only determine an upper limit fordelta(Y), whilst for the two youngest clusters in our sample (Hodge 6 and NGC1978) no conclusion about the existence of an initial He spread can be reached.Our delta(Y) estimates are consistent with the correlation between maximum Heabundance spread and mass of the host cluster found in Galactic globularclusters. This result strengthens the emerging view that the formation ofmultiple stellar populations is a standard process in massive star clusters,not limited to a high redshift environment.

Helium enrichment in intermediate-age Magellanic Clouds clusters: towards an ubiquity of multiple stellar populations?