  It is shown, using results of numerical simulations, and geophysical and
solar observations, that the transition from deterministic chaos to hard
turbulence in the magnetic field generated by the small-scale MHD dynamos
occurs through a randomization process. This randomization process has been
described using the notion of distributed chaos and the main parameter of
distributed chaos has been used for quantifying the degree of randomization.
The dissipative (Loitsianskii and Birkhoff-Saffman integrals) and ideal
(magnetic helicity) magnetohydrodynamic invariants control the randomization
process and determine the degree of randomization in different MHD flows,
directly or through the Kolmogorov-Iroshnikov phenomenology (the
magneto-inertial range of scales as a precursor of hard turbulence). Despite
the considerable differences in the scales and physical parameters, the results
of numerical simulations are in quantitative agreement with the geophysical and
solar observations in the frames of this approach. The Hall magnetohydrodynamic
dynamo has been also briefly discussed in this context.
