  Following the assumption that the disc substructures observed in
protoplanetary discs originate from the interaction between the disc and the
forming planets embedded therein, we aim to test if these putative planets
could represent the progenitors of the currently observed giant exoplanets.
  We performed N-body simulations assuming initially three, four, five or seven
planets. Our model includes pebble and gas accretion, migration, damping of
eccentricities and inclinations, disc-planet interaction and disc evolution. We
locate the planets in the positions where the gaps in protoplanetary discs have
been observed and we evolve the systems for 100Myr including a few Myr of gas
disc evolution, while also testing three values of $\alpha$ viscosity.
  For planetary systems with initially three and four planets we find that most
of the growing planets lie beyond the RV detection limit of 5AU and only a
small fraction of them migrate into the inner region. We also find that these
systems have too low final eccentricities to be in agreement with the observed
giant planet population. Systems initially consisting of five or seven planets
become unstable after $\approx$40Kyr of integration time. This clearly shows
that not every gap can host a planet. The general outcome of our simulations -
too low eccentricities - is independent of the disc's viscosity and surface
density. Further observations could either confirm the existence of an
undetected population of wide-orbit giants or exclude the presence of such
undetected population to constrain how many planets hide in gaps even further.
