Median [Fe/H] (panels a), [Mg/Fe] (panels b), and stellar age (panels c) as a function of the mean (L_z) of each cluster found in the kinematically selected halo of the solar vicinity in the four simulated galaxies (circles). The circles are colour-coded by their fraction of accreted stellar particles. The triangles represent the same quantity, but with the in situ particles removed. The vertical dashed lines located at (L_z ± 500 km s⁻¹ kpc⁻¹) indicate the separations between the retrograde, non-rotating, and prograde clusters. For the prograde clusters, the metallicity, but mostly the [Mg/Fe] and the stellar age separate well those dominated by in situ and accreted particles. However, none of those parameters is able to disentangle the clusters dominated by in situ to those dominated by accreted particles for the non-rotating and the retrograde clusters.