  The rapidly increasing number of delta Scuti stars with regular patterns
among their pulsation frequencies necessitates modelling tools to better
understand the observations. Further, with a dozen identified modes per star,
there is potential to make meaningful inferences on stellar structure using
these young $\delta$ Sct stars. We compute and describe a grid of $>$200,000
stellar models from the early pre-main-sequence to roughly one-third of the
main-sequence lifetime, and calculate their pulsation frequencies. From these,
we also calculate asteroseismic parameters and explore how those parameters
change with mass, age, and metal mass fraction. We show that the large
frequency separation, $\Delta\nu$, is insensitive to mass at the zero-age main
sequence. In the frequency regime observed, the $\Delta\nu$ we measure (from
modes with $n\sim5$--9) differs from the solar scaling relation by $\sim$13%.
We find that the lowest radial order is often poorly modelled, perhaps
indicating that the lower-order pressure modes contain further untapped
potential for revealing the physics of the stellar interior. We also show that
different nuclear reaction networks available in MESA can affect the pulsation
frequencies of young $\delta$ Sct stars by as much as 5%. We apply the grid to
five newly modelled stars, including two pre-main-sequence stars each with 15+
modes identified, and we make the grid available as a community resource.
