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The Magellanic Clouds are the most massive and closest satellite galaxies ofthe Milky Way, with stars covering ages from a few Myr up to 13 Gyr. This makesthem important for validating integrated light methods to study stellarpopulations and star-formation processes, which can be applied to more distantgalaxies. We characterized a set of stellar clusters in the Small MagellanicCloud (SMC), using the $\textit{Southern Photometric Local Universe Survey}$.This is the first age (metallicity) determination for 11 (65) clusters of thissample. Through its 7 narrow bands, centered on important spectral features,and 5 broad bands, we can retrieve detailed information about stellarpopulations. We obtained ages and metallicities for all stellar clusters usingthe Bayesian spectral energy distribution fitting code $\texttt{BAGPIPES}$.With a sample of clusters in the color range $-0.20 < r-z < +0.35$, for whichour determined parameters are most reliable, we modeled the age-metallicityrelation of SMC. At any given age, the metallicities of SMC clusters are lowerthan those of both the Gaia Sausage-Enceladus disrupted dwarf galaxy and theMilky Way. In comparison with literature values, differences are$\Delta$log(age)$\approx0.31$ and $\Delta$[Fe/H]$\approx0.41$, which iscomparable to low-resolution spectroscopy of individual stars. Finally, weconfirm a previously known gradient, with younger clusters in the center andolder ones preferentially located in the outermost regions. On the other hand,we found no evidence of a significant metallicity gradient.

Ages and metallicities of stellar clusters using S-PLUS narrow-band integrated photometry: the Small Magellanic Cloud