  Observations reveal the presence of supermassive black holes (SMBH) as early
as ~700 million years after the Big Bang. Their formation path is still subject
to current debate. We explore the influence of magnetic fields, which are
strongly amplified via the turbulent small-scale dynamo, on the formation of
SMBH seeds within the direct collapse scenario. In this study, we perform for
the first time cosmological magnetohydrodynamic large eddy simulations that
employ a model for unresolved, compressible MHD turbulence. In total we perform
36 simulations for 9 haloes each with two different initial magnetic field
strengths, and with and without employing the unresolved turbulence model. We
make use of the adaptive mesh refinement approach to achieve an effective
spatial resolution of less than one proper astronomical unit. We consider a
regime where cooling is regulated by atomic hydrogen and the molecular hydrogen
gets dissociated by a strong radiation field. Our main finding is that the
majority of the gas properties in the haloes at the final output are
predominantly determined by the run-away gravitational collapse. Turbulence is
supersonic and super-Alfv\'enic in all cases, and magnetic fields are amplified
to an approximately dynamically relevant regime. Finally, fragmentation during
the collapse is intermittent and mass accretion rates range from 0.2-3 Msun/yr.
This suggests that the presence of strongly amplified magnetic fields and
turbulence provides additional pressure support on small scales and make the
direct collapse a viable scenario for the formation of massive objects under
the required ambient conditions.
