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tokens: dex) that led us to speculate about the possibility that the assumption for young MC clusters to have metal contents similar to the mean galaxy present-day metallicities is justified for statistical purposes. Otherwise, when young clusters are studied to search for chemical abundance anomalies, light element abundance variations, binary fraction, extended main sequence turnoffs, among others, the knowledge of their actual metallicities could have an impact. This could be the case, for instance, of NGC 1844, NGC 1847, and NGC 330, for which Milone et al. ( 2013 ), Niederhofer et al. ( 2015 ) and Milone et al. ( 2018 ) adopted, respectively, more metal-rich metal abundances to show evidence of multiple populations. In order to see whether a better tracking of the split main sequences can be achieved, it would be worth trying to match their CMDs with theoretical isochrones with metallicities similar to those derived in this work. In the case of NGC 1850, a cluster with a large population of near-critically rotating stars, a slightly more metal-rich value has usually been adopted (Bastian et al. 2017 ). The existence of a spread in metallicity within the younger stellar populations of both MCs is well known. Piatti and Geisler ( 2013 ), using an homogeneous age/metallicity compilation, showed that the FWHM of such a scatter is 0.51 dex for the LMC and 0.32 dex for the SMC (see also Choudhury, Subramaniam Cole 2016 ; Choudhury et al. 2018 ); the MC cluster populations also exhibit a noticeable scatter at their younger end (see also Perren, Piatti Vázquez 2017 ). In this context, most of the present studied clusters are within the expected metallicity range, while others fall at the edge of the known metallicity distributions. This is the case of NGC 330, the most metal-poor young SMC cluster ([Fe/H] = −1.15 dex) so far. In the LMC, NGC 1847 resulted to be the most-metal poor young cluster ([Fe/H] = −0.91 dex) ever known, while NGC 1711 turned out to be at the metal-rich end of the LMC cluster’s metallicities ([Fe/H] = −0.06 dex). These relatively extreme metallicity values tell us that the gas out of which these young clusters were formed was not well mixed. Note that there has been speculations about the role of infall of unenriched (or less enriched) gas into the MCs leading to an unexpectedly large spread in cluster abundances at a relatively constant age (see e.g. Da Costa Hatzidimitriou 1998 ). We looked at the cluster positions in their respective host galaxies in order to search for any link of their derived metallicities with the chemical evolution histories of the MCs, particularly of those with more extreme values. Fig. 2 depicts with black points the spatial distributions in both MCs of all the clusters catalogued by Bica et al. ( 2008 ). The studied clusters are drawn with big filled circles. As a spatial reference, we have also included the areas defined by Harris and Zaritsky ( 2009 ) in the LMC main body (the bar is traced with a