  Gaps imaged in protoplanetary discs are suspected to be opened by planets. We
compute the present-day mass accretion rates $\dot{M}_{\rm p}$ of seven
hypothesized gap-embedded planets, plus the two confirmed planets in the PDS 70
disc. The accretion rates are based on disc gas surface densities $\Sigma_{\rm
gas}$ from C$^{18}$O observations, and planet masses $M_{\rm p}$ from
simulations fitted to observed gaps. Assuming accretion is Bondi-like, we find
in eight out of nine cases that $\dot{M}_{\rm p}$ is consistent with the
time-averaged value given by the current planet mass and system age, $M_{\rm
p}/t_{\rm age}$. As system ages are comparable to circumstellar disc lifetimes,
these gap-opening planets may be undergoing their last mass doublings, reaching
final masses of $M_{\rm p} \sim 10-10^2 \, M_\oplus$ for the non-PDS 70
planets, and $M_{\rm p} \sim 1-10 \, M_{\rm J}$ for the PDS 70 planets. For
another fifteen gaps without C$^{18}$O data, we predict $\Sigma_{\rm gas}$ by
assuming their planets are accreting at their time-averaged $\dot{M}_{\rm p}$.
Bondi accretion rates for PDS 70b and c are orders of magnitude higher than
accretion rates implied by measured U-band and H$\alpha$ fluxes, suggesting
most of the accretion shock luminosity emerges in as yet unobserved wavebands,
or that the planets are surrounded by dusty, highly extincting, quasi-spherical
circumplanetary envelopes. Thermal emission from such envelopes or from
circumplanetary discs, on Hill sphere scales, peaks at wavelengths in the
mid-to-far-infrared and can reproduce observed mm-wave excesses.
