  We investigate the properties of circumstellar discs (CDs) produced in
hydrodynamical simulations of gravoturbulent core collapse considering
Kolmogorov and Burger-type turbulence. We report that massive discs are more
prevalent in the Kolmogorov regime than for Burger-type turbulence. A
significant number of discs are formed with a radius of $\sim$ 15 au in both
cases. However, the number of extended discs with radii $>$ 15 au is
significantly larger in case of Kolmogorov turbulence. The two regimes of
turbulence, in general, yield disc radii in the ranges of 7 au $-$ 30 au, and
13 au $-$ 39 au, respectively. The corresponding ranges of the disc masses are
30.37 $M_{\rm Jup}$ $-$ 0.92 M$_{\odot}$, and 2.09 $M_{\rm Jup}$ $-$ 0.13
M$_{\odot}$, respectively. Moreover, the ratio $M_{\rm disc}$/$M_{\rm star}$ is
higher in models of Kolmogorov-type turbulence than in models of Burgers-type
turbulence. We do not find any correlation between $R_{\rm disc}$ and $M_{\rm
disc}$ over the explored range of initial temperatures (8 K $-$ 14 K) and the
type of turbulence. Also, for these initial thermal variations, the turbulent
circumstellar disc structures do not exhibit signs of turbulent diffusion.
Nonetheless, both sub and supersonic velocity dispersions cause variations in
the specific angular momentum (AM) of infalling gas, especially for CDs with
radii $\sim$ 16 au $-$ 21 au. The radial profiles of CDs do not correlate with
the initial conditions.
