  Oscillating eclipsing Algols (oEAs) are remarkable systems which allow us to
determine accurate fundamental stellar parameters (mass, radius) and probe the
stellar interiors through pulsations. TZ\,Dra is an oEA system containing a
$\delta$ Scuti component. To examine particular characteristics of such close
systems including pulsations and mass transfer, we present a detailed
photometric and spectroscopic study of TZ\,Dra. With the analysis of
high-resolution spectra, the orbital parameters were determined by the radial
velocity analysis and the atmospheric parameters were derived for the primary
component. The binary modelling and the pulsational frequency analysis was
carried out using the TESS data set. The H$\alpha$ line profiles show the
signature of mass transfer from the cool to the hot binary component. The
conclusion of mass transfer/mass loss in the system was supported by the
analysis of the orbital period changes. As a result, it was found that there is
$3.52 \times 10^{-9}$ $M_\odot$/year mass loss from the system most probably
through the hotspot and stellar winds. Additionally, most pulsation frequencies
originating from the primary component were found to be spaced by harmonics of
the orbital frequencies in particular, twelve doublets spaced by $2f_{\rm orb}$
were detected from which we infer that this star a tidally tilted pulsator. A
mean p-mode frequency spacing of $\approx 7.2 $d$^{-1}$ was found as well.
