Profiles from Run 1 at times t_O+ 0.2 kyr (i.e. just after the primary protostar appears), t_O+ 4.2 kyr, t_O+ 8.1 kyr (i.e. the stage at which the disc becomes well established), t_O+ 12.1 kyr, t_O+ 16.0 kyr and t_O+ 19.9 kyr (the end of the simulation). (a) The radial-density profile on the equatorial plane, ρ(r, z= 0). The axes are logarithmic, and a line with slope − 2.5 is shown to mimic the run of density in the disc between 10 and 200 au. The key gives the line-styles used to represent the different times. (b) The radial- temperature profile on the equatorial plane, T(r, z= 0). The axes are logarithmic, and a line with slope − 0.6 is shown to mimic the run of temperature in the disc between 10 and 200 au. (c) The radial-velocity profile on the equatorial plane, v_r(r, z= 0). The velocity axis is linear, and velocity is given in units of the local sound speed. The radius axis is logarithmic. (d) The azimuthal velocity profile on the equatorial plane, v_φ(r, z= 0). The axes are logarithmic, and lines with slopes of −1/2 and −1/4 are included to show that in the disc v_φ∝r^−1/4, corresponding to non-Keplerian differential rotation. Note that this plot has a larger radial extent than the others. (e) The radial profile of the disc aspect ratio, ⁠. Both axes are linear.