  Recently, combining high-contrast imaging and space astrometry we found that
Jupiter-like (JL) planets are frequent in the beta Pic moving group (BPMG)
around those stars where their orbit can be stable, prompting further analysis
and discussion. We broaden our previous analysis to other young nearby
associations to determine the frequency, mass, and separation of companions in
general and JL in particular and their dependencies on the mass and age of the
associations. We collected available data about companions including those
revealed by visual observations, eclipses, spectroscopy, and astrometry. We
determined search completeness and found that it is very high for stellar
companions, while completeness corrections are still large for JL companions.
Once these corrections are included, we found a high frequency of companions,
both stellar (>0.52+/-0.03) and JL (0.57+/-0.11). The two populations are
separated by a gap that corresponds to the brown dwarf desert. Within the
population of massive companions, we found trends in frequency, separation, and
mass ratios with stellar mass. Planetary companions pile up in the region just
outside the ice line and we found them to be frequent once completeness was
considered. The frequency of JL planets decreases with the overall mass and
possibly the age of the association. We tentatively identify the two
populations as due to disk fragmentation and core accretion, respectively. The
distributions of stellar companions with a semi-major axis <1000 au is well
reproduced by a simple model of formation by disk fragmentation. The observed
trends with stellar mass can be explained by a shorter but much more intense
phase of accretion onto the disk of massive stars and by a more steady and
prolonged accretion on solar-type stars. Possible explanations for the trends
in the population of JL planets with association mass and age are briefly
discussed.
