We study the mass-to-flux ratio M/Φ of clumps and cores in simulations of supersonic, magnetohydrodynamical turbulence for different initial magnetic field strengths. We investigate whether the M/Φ of core and envelope, can be used to distinguish between theories of ambipolar diffusion and turbulence-regulated star formation. We analyse for different lines of sight (LoSs) in various subcubes of our simulation box. We find that (1) the average and median values of for different times and initial magnetic field strengths are typically ≳1; (2) the average and median values of saturate at for smaller magnetic fields; and (3) values of for small magnetic fields in the envelope are caused by field reversals when turbulence twists the field lines such that field components in different directions average out. Finally, we propose two mechanisms for generating values for the weak and strong magnetic field limits in the context of a turbulent model. First, in the weak field limit, the small-scale turbulent dynamo leads to a significantly increased flux in the core and we find . Secondly, in the strong field limit, field reversals in the envelope also lead to values . These reversals are less likely to occur in the core region where the velocity field is more coherent and the internal velocity dispersion is typically subsonic.