  In 2015, we initiated a survey of Scorpius-Centaurus A-F stars that are
predicted to host warm-inner and cold-outer belts of debris similar to the case
of the system HR~8799. The survey aims to resolve the disks and detect planets
responsible for the disk morphology. In this paper, we study the F-type star
HIP~67497 and present a first-order modelisation of the disk in order to derive
its main properties. We used the near-infrared integral field spectrograph
(IFS) and dual-band imager IRDIS of VLT/SPHERE to obtain angular-differential
imaging observations of the circumstellar environnement of HIP~67497. We
removed the stellar halo with PCA and TLOCI algorithms. We modeled the disk
emission with the GRaTeR code. We resolve a ring-like structure that extends up
to $\sim$450 mas ($\sim$50 au) from the star in the IRDIS and IFS data. It is
best reproduced by models of a non-eccentric ring with an inclination of
$80\pm1^{\circ}$, a position angle of $-93\pm1^{\circ}$, and a semi-major axis
of $59\pm3$ au. We also detect an additional, but fainter, arc-like structure
with a larger extension (0.65 arcsec) South of the ring that we model as a
second belt of debris at $\sim$130 au. We detect 10 candidate companions at
separations $\geq$1''. We estimate the mass of putative perturbers responsible
for the disk morphology and compare it to our detection limits. Additional data
are needed to find those perturbers, and to relate our images to large-scale
structures seen with HST/STIS.
