Global properties of the clusters and gas over time for models M4 (orange), M5 (maroon), and M6 (blue-violet) in units of free-fall time t_ff of the initial cloud (given in Table 1). From top left to bottom right: (a) SFR, where the transparent lines show the SFR at each star formation event, and the solid lines give the SFR smoothed using a Gaussian filter with σ = 0.005t_ff. (b) Instantaneous and integrated SFEs of the clouds, where ϵ_inst = M_⋆/(M_gas + M_sink + M_⋆) and ϵ_int = M_⋆/M_cloud = ϵ_⋆. (c) Most massive star formed. (d) Number of formed stars. Dashed line: actual number of stars that would form from sampling the IMF given the amount of gas mass collected for star formation by sink particles. Solid line: number of stars followed in TORCH after the sampled stellar population below 4 M_⊙ has been agglomerated. Dotted line: number of stars above 20 M_⊙ on the grid that are generating feedback. The number of stars can drop due to SN, mass loss, or exiting the grid. (e) 3D stellar velocity dispersion. (f) Half-mass radius of the entire star cluster. (g) Total mass (dotted line), mass of stars (dashed line) and gas (solid line) on the grid. (h) Virial parameter of stars (dashed line) and gas (solid line), where α_v = 0.5 is the equilibrium value. (i) Fraction of mass bound for stars (dashed line) and gas (solid line).