  Studies during the last decade have revealed that nearly all Globular
Clusters (GCs) host multiple populations (MPs) of stars with a distinctive
chemical patterns in light elements. No evidence of such MPs has been found so
far in lower-mass ($< \sim 10^4$ M$_{\odot}$) open clusters nor in intermediate
age (1-2 Gyr) massive ($> 10^5$ M$_{\odot}$) clusters in the Local Group. Young
massive clusters (YMCs) have masses and densities similar to those expected of
young GCs in the early universe, and their near-infrared (NIR) spectra are
dominated by the light of red super giants (RSGs). The spectra of these stars
may be used to determine the cluster's abundances, even though the individual
stars cannot be spatially resolved from one another. We carry out a
differential analysis between the Al lines of YMC NGC 1705: 1 and field Small
Magellanic Cloud RSGs with similar metallicities. We exclude at high confidence
extreme [Al/Fe] enhancements similar to those observed in GCs like NGC 2808 or
NGC 6752. However, smaller variations cannot be excluded.
