  Planets are born from disks of gas and dust, and observations of
protoplanetary disks are used to constrain the initial conditions of planet
formation. However, dust mass measurements of Class II disks with ALMA have
called into question whether they contain enough solids to build the exoplanets
that have been detected to date. In this paper, we calculate the mass and
spatial scale of solid material around Sun-like stars probed by transit and
radial velocity exoplanet surveys, and compare those to the observed dust
masses and sizes of Class II disks in the same stellar mass regime. We show
that the apparent mass discrepancy disappears when accounting for observational
selection and detection biases. We find a discrepancy only when the planet
formation efficiency is below 100%, or if there is a population of undetected
exoplanets that significantly contributes to the mass in solids. We identify a
positive correlation between the masses of planetary systems and their
respective orbital periods, which is consistent with the trend between the
masses and the outer radii of Class II dust disks. This implies that, despite a
factor 100 difference in spatial scale, the properties of protoplanetary disks
seem to be imprinted on the exoplanet population.
