Comparison of cluster age, t (left), and metallicity, Z (right), derived from SPS models with rotation and literature results of clusters in WAGGS (Usher et al. 2017). The spectrum fitting was based on the wavelength range 3700 ≤ λ/@@@ ≤ 5000. For this comparison, we selected clusters of interest from the Large and Small Magellanic Clouds. The horizontal axis presents the values collected from Mucciarelli et al. (2007, 2011, 2008, 2012), Glatt et al. (2009), Bastian & Silva-Villa (2013), Goudfrooij et al. (2014), and Niederhofer et al. (2015). Different colors represent different clusters, and markers represent SPS models with various rotation rates. The median values of the best-fit metallicity are shown for each cluster. Both the cluster age and metallicity exhibit a one-to-one correlation (gray dashed line) with the literature results. An age uncertainty of 0.1 dex (25%) is shown in the left panel as dash-dotted lines. NGC 2136 shares the same location as NGC 1850.