  Whether the angular momentum of protoplanetary discs is redistributed by
viscosity or extracted by magnetised winds is a long-standing question.
Demographic indicators, such as gas disc sizes and stellar accretion rates,
have been proposed as ways of distinguishing between these two mechanisms. In
this paper, we implement one-dimensional gas simulations to study the evolution
of "hybrid" protoplanetary discs simultaneously driven by viscosity and
magnetised winds, with dead zones present. We explore how the variations of
disc properties, including initial disc sizes, dead zone sizes and angular
momentum transport efficiency, affect stellar accretion rates, disc surface
density profiles, disc sizes, disc lifetimes, and cumulative mass loss by
different processes. Our models show that the expansion of the gas disc size
can be sustained when the majority of angular momentum is removed by the
magnetised wind for individual protoplanetary discs. However, when we can only
observe discs via demographic screenshots, the variation of disc sizes with
time is possibly diminished by the disc "personalities", by which we mean the
variations of initial disc properties among different discs. Our "hybrid"
models re-assess association of the two demographic indicators with mechanisms
responsible for angular momentum transport and suggest additional diagnostics
are required to assist the differentiation.
