  The Cygnus region hosts one of the most remarkable star-forming regions in
the Milky Way. Indeed, the total mass in molecular gas of the Cygnus X complex
exceeds 10 times the total mass of all other nearby star-forming regions.
Surveys at all wavelengths, from radio to gamma-rays, reveal that Cygnus
contains such a wealth and variety of sources---supernova remnants (SNRs),
pulsars, pulsar wind nebulae (PWNe), H II regions, Wolf-Rayet binaries, OB
associations, microquasars, dense molecular clouds and superbubbles---as to
practically be a galaxy in microcosm. The gamma-ray observations along reveal a
wealth of intriguing sources at energies between 1 GeV and tens of TeV.
However, a complete understanding of the physical phenomena producing this
gamma-ray emission first requires us to disentangle overlapping sources and
reconcile discordant pictures at different energies. This task is made more
challenging by the limited angular resolution of instruments such as the Fermi
Large Area Telescope, ARGO-YBJ, and HAWC and the limited sensitivity and field
of view of current imaging atmospheric Cherenkov telescopes (IACTs). The
Cherenkov Telescope Array (CTA), with its improved angular resolution, large
field of view, and order of magnitude gain in sensitivity over current IACTs,
has the potential to finally create a coherent and well-resolved picture of the
Cygnus region between a few tens of GeV and a hundred TeV. We describe a
proposed strategy to study the Cygnus region using CTA data, which combines a
survey of the whole region at $65^{\circ} < l < 85^{\circ}$ and $-3.5^{\circ} <
b < 3.5^{\circ} $ with deeper observations of two sub-regions that host rich
groups of known gamma-ray sources.
