  Comprehensive spectral analyses of the Galactic Wolf-Rayet stars of the
nitrogen sequence (i.e.\ the WN subclass) have been performed in a previous
paper. However, the distances of these objects were poorly known. Distances
have a direct impact on the "absolute" parameters, such as luminosities and
mass-loss rates. The recent Gaia Data Release (DR2) of trigonometric parallaxes
includes nearly all WN stars of our Galactic sample. In the present paper, we
apply the new distances to the previously analyzed Galactic WN stars and
rescale the results accordingly. On this basis, we present a revised catalog of
55 Galactic WN stars with their stellar and wind parameters. The correlations
between mass-loss rate and luminosity show a large scatter, for the
hydrogen-free WN stars as well as for those with detectable hydrogen. The
slopes of the $\log L - \log \dot{M}$ correlations are shallower than found
previously. The empirical Hertzsprung-Russell diagram (HRD) still shows the
previously established dichotomy between the hydrogen-free early WN subtypes
that are located on the hot side of the zero-age main sequence (ZAMS), and the
late WN subtypes, which show hydrogen and reside mostly at cooler temperatures
than the ZAMS (with few exceptions). However, with the new distances, the
distribution of stellar luminosities became more continuous than obtained
previously. The hydrogen-showing stars of late WN subtype are still found to be
typically more luminous than the hydrogen-free early subtypes, but there is a
range of luminosities where both subclasses overlap. The empirical HRD of the
Galactic single WN stars is compared with recent evolutionary tracks. Neither
these single-star evolutionary models nor binary scenarios can provide a fully
satisfactory explanation for the parameters of these objects and their location
in the HRD.
