  Remnant accretion disks formed in compact object mergers are an important
ingredient in the understanding of electromagnetic afterglows of
multi-messenger gravitational-wave events. Due to magnetically and neutrino
driven winds, a significant fraction of the disk mass will eventually become
unbound and undergo r-process nucleosynthesis. While this process has been
studied in some detail, previous studies have typically used approximate
initial conditions for the accretion disks, or started from purely
hydrodynamical simulations. In this work, we analyse the properties of
accretion disks formed from near equal-mass black hole-neutron star mergers
simulated in general-relativistic magnetohydrodynamics in dynamical spacetimes
with an accurate microphysical description. The post-merger systems were
evolved until $120\, {\rm ms}$ for different finite-temperature equations of
state and black-hole spins. We present a detailed analysis of the fluid
properties and of the magnetic-field topology. In particular, we provide
analytic fits of the magnetic-field strength and specific entropy as a function
of the rest-mass density, which can be used for the construction of equilibrium
disk models. Finally, we evolve one of the systems for a total of $350\, \rm
ms$ after merger and study the prospect for eventual jet launching. While our
simulations do not reach this stage, we find clear evidence of continued funnel
magnetization and clearing, a prerequisite for any jet-launching mechanism.
