  We report the APOGEE-2S$+$ discovery of a unique collection of
nitrogen-enhanced mildly metal-poor giant stars, peaking at [Fe/H]$\sim -0.89$
with no carbon enrichment, toward the Small and Large Magellanic Clouds (MCs),
with abundances of light- (C, N), odd-Z (Al, K) and $\alpha-$elements (O, Mg,
Si) that are typically found in Galactic globular clusters (GCs). Here we
present 44 stars in the MCs that exhibit significantly enhanced [N/Fe]
abundance ratios, well above ([N/Fe]$>+0.6$) typical Galactic levels at similar
metallicity, and a star that is very nitrogen-enhanced ([N/Fe]$> +2.45$). Our
sample consists of luminous evolved stars on the asymptotic giant branch (AGB),
eight of which are classified as bonafide semi-regular (SR) variables, as well
as low-luminosity stars similar to that of stars on the tip of the red giant
branch of stellar clusters in the MCs. It seems likely that whatever
nucleosynthetic process is responsible for these anomalous MC stars it is
similar to that which caused the common stellar populations in GCs. We
interpret these distinctive C-N patterns as the observational evidence of the
result of tidally shredded GCs in the MCs. These findings might explain some
previous conflicting results over bulge N-rich stars, and broadly help to
understand GC formation and evolution. Furthermore, the discovery of such a
large population of N-rich AGB stars in the MCs suggests that multiple stellar
populations might not only be exotic events from the past but can also form at
lower redshift.
