  We study the relative helicity of active region (AR) NOAA~12673 during a
ten-hour time interval centered around a preceding X2.2 flare
(SOL2017-09-06T08:57) and also including an eruptive X9.3 flare that occurred
three hours later (SOL2017-09-06T11:53). In particular, we aim for a reliable
estimate of the normalized self-helicity of the current-carrying magnetic
field, the so-called helicity ratio $|H_{\mathrm{J}}|/|H_{\mathcal{V}}|$, a
promising candidate to quantity the eruptive potential of solar ARs. Using
SDO/HMI vector magnetic field data as an input, we employ nonlinear force-free
(NLFF) coronal magnetic field models using an optimization approach. The
corresponding relative helicity, and related quantities, are computed using a
finite-volume method. From multiple time series of NLFF models based on
different choices of free model parameters, we are able to assess the spread of
$|H_{\mathrm{J}}|/|H_{\mathcal{V}}|$, and to estimate its uncertainty. In
comparison to earlier works, which identified the non-solenoidal contribution
to the total magnetic energy, $E_{\rm div}/E$, as selection criterion regarding
the required solenoidal quality of magnetic field models for subsequent
relative helicity analysis, we propose to use in addition the non-solenoidal
contribution to the free magnetic energy, $|E_{\rm mix}|/E_{\mathrm{J,s}}$. As
a recipe for a reliable estimate of the relative magnetic helicity (and related
quantities), we recommend to employ multiple NLFF models based on different
combinations of free model parameters, to retain only those that exhibit
smallest values of both $E_{\rm div}/E$ and $|E_{\rm mix}|/E_{\mathrm{J,s}}$ at
a certain time instant, to subsequently compute mean estimates, and to use the
spread of the individually contributing values as an indication for the
uncertainty.
