  Context: Several observations of the local Universe (LU) point towards the
existence of very prominent structures. The presence of massive galaxy clusters
and local super clusters on the one hand, but also large local voids and
under-densities on the other hand. However, it is highly non trivial to connect
such different observational selected tracers to the underlying dark matter
(DM) distribution. Methods (abridged): We used a 500 Mpc/h large constrained
simulation of the LU with initial conditions based on peculiar velocities
derived from the CosmicFlows-2 catalogue and follow galaxy formation physics
directly in the hydro-dynamical simulations to base the comparison on stellar
masses of galaxies or X-ray luminosity of clusters. We also used the 2668 Mpc/h
large cosmological box from the Magneticum simulations to evaluate the
frequency of finding such anomalies in random patches within simulations.
Results: We demonstrate that haloes and galaxies in our constrained simulation
trace the local DM density field very differently. Thereby, this simulation
reproduces the observed 50% under-density of galaxy clusters and groups within
the sphere of ~100 Mpc when applying the same mass or X-ray luminosity limit
used in the observed cluster sample (CLASSIX), which is consistent with a
~1.5$\sigma$ feature. At the same time, the simulation reproduces the observed
over-density of massive galaxy clusters within the same sphere, which on its
own also corresponds to a ~1.5$\sigma$ feature. Interestingly, we find that
only 44 out of 15635 random realizations (i.e. 0.28%) are matching both
anomalies, making the LU to be a ~3$\sigma$ environment. We finally compared a
mock galaxy catalogue with the observed distribution of galaxies in the LU,
finding also a match to the observed factor of two over-density at ~16 Mpc as
well as the observed 15% under-density at ~40 Mpc distance.
