  We report the detection, made using ALMA, of the 92 GHz continuum and
hydrogen recombination lines (HRLs) H40$\alpha$, H42$\alpha$, and H50$\beta$
emission toward the ionized wind associated with the high-mass young stellar
object G345.4938+01.4677. This is the luminous central dominating source
located in the massive and dense molecular clump associated with IRAS
16562$-$3959. The HRLs exhibit Voigt profiles, a strong signature of Stark
broadening. We successfully reproduce the observed continuum and HRLs
simultaneously using a simple model of a slow ionized wind in local
thermodynamic equilibrium, with no need a high-velocity component. The
Lorentzian line wings imply electron densities of $5\times10^7$ cm$^{-3}$ on
average. In addition, we detect SO and SO$_2$ emission arising from a compact
($\sim3000$ AU) molecular core associated with the central young star. The
molecular core exhibits a velocity gradient perpendicular to the jet-axis,
which we interpret as evidence of rotation. The set of observations toward
G345.4938+01.4677 are consistent with it being a young high-mass star
associated with a slow photo-ionized wind.
