  The Asymptotic Giant Branch (AGB) scenario ascribes the multiple populations
in old Galactic Globular Clusters (GGC) to episodes of star formation in the
gas contaminated by the ejecta of massive AGBs and super-AGBs of a first
stellar population. The mass of these AGBs (4-8Msun) today populate the Young
Massive Clusters (YMC) of the Magellanic Clouds, where rapid rotation and its
slowing down play an important role in shaping the color magnitude diagram
features. Consequently, we must reconsider whether the rotational evolution of
these masses affects the yields, and whether the resulting abundances are
compatible with the chemical patterns observed in GGC. We show the first
results of a differential analysis, by computing the hot bottom burning
evolution of non rotating models with increased CNO-Na abundances at the 2DU,
following the results of MESA rotational models.
