  We present a comprehensive radiative magnetohydrodynamic simulation of the
quiet Sun and large solar active regions. The 197 Mm wide simulation domain
spans from 18 (10) Mm beneath the photosphere to 113 Mm in the solar corona.
Radiative transfer assuming local thermal equilibrium, optically-thin radiative
losses, and anisotropic conduction transport provide the necessary realism for
synthesizing observables to compare with remote sensing observations of the
photosphere and corona. This model self-consistently reproduces observed
features of the quiet Sun, emerging and developed active regions, and solar
flares up to M class. Here, we report an overview of the first results. The
surface magnetoconvection yields an upward Poynting flux that is dissipated in
the corona and heats the plasma to over one million K. The quiescent corona
also presents ubiquitous propagating waves, jets, and bright points with sizes
down to 2 Mm. Magnetic flux bundles emerge into the photosphere and give rise
to strong and complex active regions with over $10^{23}$ Mx magnetic flux. The
coronal free magnetic energy, which is approximately 18\% of the total magnetic
energy, accumulates to approximately $10^{33}$ erg. The coronal magnetic field
is clearly non-force-free, as the Lorentz force needs to balance the pressure
force and viscous stress as well as drive magnetic field evolution. The
emission measure from $\log_{10}T{=}4.5$ to $\log_{10}T{>}7$ provides a
comprehensive view of the active region corona, such as coronal loops of
various lengths and temperatures, mass circulation by evaporation and
condensation, and eruptions from jets to large-scale mass ejections.
