  As our closest cluster-neighbor, the Virgo cluster of galaxies is intensely
studied by observers to unravel the mysteries of galaxy evolution within
clusters. At this stage, cosmological numerical simulations of the cluster are
useful to efficiently test theories and calibrate model. However, it is not
trivial to select the perfect simulacrum of the Virgo cluster to fairly compare
in detail its observed and simulated galaxy populations that are affected by
the type and history of the cluster. Determining precisely the properties of
Virgo for a later selection of simulated clusters becomes essential. It is
still not clear how to access some of these properties such as the past history
of the Virgo cluster from current observations. Therefore, directly producing
effective simulacra of the Virgo cluster is inevitable. Efficient simulacra of
the Virgo cluster can be obtained via simulations that resemble the local
Universe down to the cluster scale. In such simulations, Virgo-like halos form
in the proper local environment and permit assessing the most probable
formation history of the cluster. Studies based on these simulations have
already revealed that the Virgo cluster has had a quiet merging history over
the last seven gigayears and that the cluster accretes matter along a
preferential direction. This paper reveals that in addition such Virgo halos
have had on average only one merger larger than about a tenth of their mass at
redshift zero within the last four gigayears. This second branch (by opposition
to main branch) formed in a given sub-region and merged recently (within the
last gigayear). These properties are not shared with a set of random halos
within the same mass range. This study extends [truncated]
