  High-mass multiples might form via fragmentation of self-gravitational disks
or alternative scenarios such as disk-assisted capture. However, only few
observational constraints exist on the architecture and disk structure of
high-mass protobinaries and their accretion properties. Here we report the
discovery of a close ($57.9\pm0.2$mas=170au) high-mass protobinary,
IRAS17216-3801, where our VLTI/GRAVITY+AMBER near-infrared interferometry
allows us to image the circumstellar disks around the individual components
with 3 milliarcsecond resolution. We estimate the component masses to $\sim20$
and $\sim18 M_{\odot}$ and find that the radial intensity profiles can be
reproduced with an irradiated disk model, where the inner regions are excavated
of dust, likely tracing the dust sublimation region in these disks. The
circumstellar disks are strongly misaligned with respect to the binary
separation vector, which indicates that the tidal forces did not have time to
realign the disks, pointing towards a young dynamical age of the system. We
constrain the distribution of the Br$\gamma$ and CO-emitting gas using
VLTI/GRAVITY spectro-interferometry and VLT/CRIRES spectro-astrometry and find
that the secondary is accreting at a higher rate than the primary. VLT/NACO
imaging shows $L'$-band emission on 3-4 times larger scales than the binary
separation, matching the expected dynamical truncation radius for the
circumbinary disk. The IRAS17216-3801 system is $\sim3\times$ more massive and
$\sim5\times$ more compact than other high-mass multiplies imaged at infrared
wavelengths and the first high-mass protobinary system where circumstellar and
circumbinary dust disks could be spatially resolved. This opens exciting new
opportunities for studying star-disk interactions and the role of multiplicity
in high-mass star formation.
