  Detailed understanding of stellar physics is essential towards a robust
determination of stellar properties (e.g. radius, mass, and age). Among the
vital input physics used in the modelling of solar-type stars which remain
poorly constrained, is the initial helium abundance. To this end, when
constructing stellar model grids, the initial helium abundance is estimated
either (i) by using the semi-empirical helium-to-heavy element enrichment
ratio, (${\Delta Y}/{\Delta Z}$), anchored to the standard Big Bang
Nucleosynthesis value or (ii) by setting the initial helium abundance as a free
variable. Adopting 35 low-mass, solar-type stars with multi-year Kepler
photometry from the asteroseismic "LEGACY" sample, we explore the systematic
uncertainties on the inferred stellar parameters (i.e., radius, mass, and age)
arising from the treatment of the initial helium abundance in stellar model
grids . The stellar masses and radii derived from grids with free initial
helium abundance are lower compared to those from grids based on a fixed
${\Delta Y}/{\Delta Z}$ ratio. We find the systematic uncertainties on mean
density, radius, mass, and age arising from grids which employ a fixed value of
${\Delta Y}/{\Delta Z}$ and those with free initial helium abundance to be
$\sim$ 0.9%, $\sim$ 2%, $\sim$ 5% and $\sim$ 29%, respectively. We report that
the systematic uncertainties on the inferred masses and radii arising from the
treatment of initial helium abundance in stellar grids lie within the expected
accuracy limits of ESA's PLATO, although this is not the case for the age.
