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The color-magnitude diagrams of many Magellanic Cloud clusters (with ages upto 2 billion years) display extended turnoff regions where the stars leave themain sequence, suggesting the presence of multiple stellar populations withages which may differ even by hundreds million years (Mackey et al. 2008,Milone et al. 2009, Girardi et al. 2011). A strongly debated question iswhether such an extended turnoff is instead due to populations with differentstellar rotations (Girardi et al. 2011, Goudfrooij et al. 2011, Rubele et al.2013, Li et al. 2014). The recent discovery of a `split' main sequence in someyounger clusters (about 80--400Myr) added another piece to this puzzle. Theblue (red) side of the main sequence is consistent with slowly (rapidly)rotating stellar models (D'Antona et al. 2015, Milone et al. 2016, Correnti etal. 2017, Milone et al 2016), but a complete theoretical characterization ofthe observed color-magnitude diagram appeared to require also an age spread(Correnti et al. 2017). We show here that, in three clusters so far analyzed,if the blue main sequence stars are interpreted with models that have beenalways slowly rotating, they must be about 30% younger than the rest of thecluster. If they are instead interpreted as stars initially rapidly rotating,but that have later slowed down, the age difference disappears, and "braking"also helps to explain the apparent age differences of the extended turnoff. Theage spreads in Magellanic Cloud clusters are a manifestation of rotationalstellar evolution. Observational tests are suggested.

Stars caught in the braking stage in young Magellanic Clouds clusters