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The Magellanic Clouds host a large population of massive (> 10^4 Msun) starclusters with ages ranging from a few Myr to 12 Gyr. In nearly all cases, closeinspection of their CMDs reveals features that deviate from expectations of aclassic isochrone. Young (< 2 Gyr) clusters show extended main sequenceturnoffs and in some cases split/dual main sequences. Clusters older than ~ 2Gyr show splitting in the red giant branches when viewed in UV filters that aresensitive to abundance variations (in particular nitrogen). A distribution ofstellar rotation rates appears to be the cause of the complex features observedin the young and intermediate age clusters, while above ~ 2 Gyr the featuresseem to be the same light-element abundance variations as observed in theancient Galactic globular clusters, a.k.a. "multiple populations". Here, weprovide an overview of current observations and their interpretations andsummarise possible links between all the classes of complexities, regardless ofage.

Interpreting the complex CMDs of the Magellanic Clouds clusters