Relationship between the maximum stellar mass (M_max), the Plummer radius (a_pl) and the EFF scale radius (a_eff) at 4t_ff, and the velocity dispersion (σ_v) for simulations at refinement level 3 with different random seeds. All quantities are measured using stars within the radius around the densest region of the cluster that encloses 95% of the total stellar mass. The green line shows a linear fit to a_pl (plus symbols), given by a_pl/(1pc) = (0.0091 ± 0.0041)[M_max/(1 M_⊙)] + 0.1608. The magenta line shows a linear fit to a_eff (circle symbols), given by a_eff/(1 pc) = (0.0084 ± 0.0035)[M_max/(1 M_⊙)] − 0.0437. The blue line shows a linear fit to σ_v (square symbols), given by σv/(1kms⁻¹) = (−0.017 8 ± 0.0051)[M_max/(1 M_⊙)] + 2.6391. These linear fits are obtained with the linregress function from scipy.stats, which applies ordinary least-squares regression. The upper y-axis corresponds to a_pl and a_eff in parsecs, while the lower y-axis represents σ_v in km s⁻¹.