  Asteroseismology is a powerful tool to infer fundamental stellar properties.
The use of these asteroseismic-inferred properties in a growing number of
astrophysical contexts makes it vital to understand their accuracy.
Consequently, we performed a hare-and-hounds exercise where the hares simulated
data for 6 artificial main-sequence stars and the hounds inferred their
properties based on different inference procedures. To mimic a pipeline such as
that planned for the PLATO mission, all hounds used the same model grid. Some
stars were simulated using the physics adopted in the grid, others a different
one. The maximum relative differences found (in absolute value) between the
inferred and true values of the mass, radius, and age were 4.32 per cent, 1.33
per cent, and 11.25 per cent, respectively. The largest systematic differences
in radius and age were found for a star simulated assuming gravitational
settling, not accounted for in the model grid, with biases of -0.88 per cent
(radius) and 8.66 per cent (age). For the mass, the most significant bias
(-3.16 per cent) was found for a star with a helium enrichment ratio outside
the grid range. Moreover, a ~7 per cent dispersion in age was found when
adopting different prescriptions for the surface corrections or shifting the
classical observations by $\pm 1\sigma$. The choice of the relative weight
given to the classical and seismic constraints also impacted significantly the
accuracy and precision of the results. Interestingly, only a few frequencies
were required to achieve accurate results on the mass and radius. For the age
the same was true when at least one $l=2$ mode was considered.
