  HD\,139614 is known to be a $\sim$14-Myr-old, possibly pre-main-sequence star
in the Sco-Cen OB association in the Upper Centaurus-Lupus subgroup, with a
slightly warped circumstellar disc containing ring structures hinting at one or
more planets. The star's chemical abundance pattern is metal-deficient except
for volatile elements, which places it in the $\lambda$ Boo class and suggests
it has recently accreted gas-rich but dust-poor material. We identify seven
dipole and four radial pulsation modes among its $\delta$ Sct pulsations using
the TESS light curve and an \'echelle diagram. Precision modelling with the
MESA stellar evolution and GYRE stellar oscillation programs confirms it is on
the pre-main sequence. Asteroseismic, grid-based modelling suggests an age of
$10.75\pm0.77$ Myr, a mass of $1.52\pm0.02$ M$_{\odot}$, and a global metal
abundance of $Z=0.0100\pm0.0010$. This represents the first asteroseismic
determination of the bulk metallicity of a $\lambda$ Boo star. The precise age
and metallicity offer a benchmark for age estimates in Upper Centaurus--Lupus,
and for understanding disc retention and planet formation around
intermediate-mass stars.
