  We report on the magnitude of the intrinsic [Fe/H] spread in the Small
Magellanic Cloud (SMC) intermediate-age massive clusters NGC 339, 361, Lindsay
1 and 113, respectively. In order to measure the cluster metallicity
dispersions, we used accurate Stromgren photometry of carefully selected
cluster red giant branch (RGB) stars. We determined the Fe-abundance spreads by
employing a maximum likelihood approach. The spreads obtained using the more
accurate photometry of the brighter RGB stars resulted to be marginal (~
0.05+-0.03 dex) for NGC 339 and NGC 361, while for Lindsay 1 and Lindsay 113 we
obtained metallicity spreads of 0.00+-0.04 dex. From these results, we
speculated with the possibility that NGC 361 is added to the group of four SMC
clusters with observational evidence of multiple populations (MPs).
Furthermore, in the context of the present debate about the existence of
Fe-abundance inhomogeneities among old clusters with MPs, these outcomes put
new constrains to recent theoretical speculations for making this phenomenon
visible.
