Panel a: rest-frame 1.4 GHz radio luminosity (L_{1.4 GHz}, bottom axis) and 1.4 GHz SFR (SFR_{1.4 GHz}, top axis) distributions for the LERGs, HERGs, and SFGs in XXL-S. LERGs and RL HERGs are found at all radio luminosities, but RL HERGs tend to have higher luminosities. The SFGs and RQ HERGs are cut off at at L_{1.4 GHz} < 10^24.5 W Hz⁻¹ because of the radio luminosity requirement for radio AGN. The high SFR_{1.4 GHz} values for LERGs and RL HERGs (≳10^3.3 M_⊙ yr⁻¹) are due to AGN contamination in their radio emission. Panel b: MAGPHYS stellar mass (M_*) distribution for the LERGs, HERGs, and SFGs in XXL-S. The host galaxies of LERGs have median M_* ≈ 10^11.06 M_⊙, whereas HERGs and SFGs tend to be hosted by galaxies of lower median stellar mass (median M_* ≈ 10^10.6 –10^10.8 M_⊙). Panel c: MAGPHYS star formation rate (SFR_MP) distribution for the LERGs, HERGs, and SFGs in XXL-S. LERGs exhibit low median SFRs (~2 M_⊙ yr⁻¹) compared to that of HERGs and SFGs (~12–17 M_⊙ yr⁻¹). Panel d: NUV − u colour distribution for the LERGs, HERGs, and SFGs in XXL-S. The colours were derived from the MAGPHYS SED fitting. LERGs have redder median colours (NUV − u ≈ 2.21) than RL HERGs (NUV − u ≈ 0.99), RQ HERGs (NUV − u ≈ 1.12), and SFGs (NUV − u ≈ 1.25).