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tokens: that for the initial core as a whole (β core = 1.9), is much smaller than what is typically adopted in MHD simulations of protoplanetary discs, as mentioned earlier. Interestingly, the magnetic energy is dominated by the poloidal component of the magnetic field rather than the toroidal component, as shown by the values of β t and β p in Fig. 15 for each disc, which are the ratios of the thermal to magnetic energy due to the toroidal and poloidal field component, respectively. The disc remains significantly magnetized at later epochs. The values of λ d and β are formally 9.2 and 2.5, respectively, at the epoch when , smaller than their counterparts at the earlier epoch of , but they are affected by a relatively low-density region that satisfies the disc criteria but is detached from the main body of the disc (see panel v of Fig. 15 ). By the last epoch shown (panel aa, ), the disc has λ d = 23 and β = 7.7, with the magnetic energy strongly dominated by the poloidal field component. As the AD coefficient increases, the disc starts to form earlier. For example, by the epoch when , a disc is already well-developed in the most magnetically diffusive model (M0.0AD10.0, panel l), clearly visible although underdeveloped in the second most diffusive model (M0.0AD3.0, panel k), but barely discernible in the standard AD case (panel j). Another trend is that, as the AD coefficient increases, the disc is somewhat bigger (compare the discs in the last three columns of Fig. 15 ) and more massive, with the disc mass increasing from for Model M0.0AD1.0 to for M0.0AD3.0 to for M0.0AD10.0. The disc remains significantly magnetized, with λ d ∼ 10−20 and β ∼ 10−20 typically, and the magnetic energy dominated by the poloidal field component in most cases. The main exception is the last epoch of the most diffusive model (M0.0AD10.0, ), when the disc is significantly less magnetized, with λ d = 32, β = 59, and the magnetic energy dominated by the toroidal field component instead. Turbulence changes the formation and properties of discs substantially, as illustrated by Fig. 16 , which is the same as Fig. 15 but for all models with sonic turbulence () and different levels of AD. The change is the most pronounced at the earliest epoch (), when the disc is well developed in all AD models and is clearly visible (although underdeveloped) even for the ideal MHD case (panel a). The ideal MHD disc is strongly magnetized, with λ d = 3.8 that is comparable to that of its parental core (especially the central part that is less magnetized compared to the core as a whole) and a plasma-β that is much less than unity (β d = 0.1). The strong magnetization, we believe, is the reason that the disc enabled by turbulence early in the ideal MHD case is transient; the magnetic braking is simply too efficient to allow the disc to persist for a long time. The same is broadly true for the early discs formed in the two weakest AD cases (Model M1.0AD0.1 and M1.0AD0.3), even though their masses